| GOES 12 | GOES 10 |
| Cur | 1904 | M2.3 | Ratio 0.106 | 1904 | M2.4 | Ratio 0.095 | ||
| Beg | 1703 | C8.2 | 1703 | C7.7 | ||||
| Max | 1725 | X9.2 | Int 9.99e-01 J m-2 | 1725 | X8.3 | Int 9.05e-01 J m-2 | ||
| End | 1739 | X4.4 | 1739 | X4.0 |
| GOES 12 | GOES 10 |
| Cur | 1904 | M2.3 | Ratio 0.106 | 1904 | M2.4 | Ratio 0.095 | ||
| Beg | 1703 | C8.2 | 1703 | C7.7 | ||||
| Max | 1725 | X9.2 | Int 9.99e-01 J m-2 | 1725 | X8.3 | Int 9.05e-01 J m-2 | ||
| End | 1739 | X4.4 | 1739 | X4.0 |
This GOES X-ray flux plot contains 1 minute averages of solar X-ray output in the 1-8 Angstrom (0.1-0.8 nm) and 0.5-4.0 Angstrom (0.05-0.4 nm) passbands. Data from both operational GOES satellites are included. Some data dropouts will occur during satellite eclipses. SEC alerts are issued at the M5 (5x10E-5 Watts/m2) and X1 (1x10E-4 Watts/m2) levels, based upon 1-minute data. Large X-ray bursts cause short wave fades for HF propagation paths through the sunlit hemisphere. Some large flares are accompanied by strong solar radio bursts that may interfere with satellite downlinks.
